adsabs/AstroCLIMB huggingface dataset:
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Dependencies of the reaction rate ﹩{r}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{\rm{H}}{\rm{D}}}﹩ on number density [g - HD] measured at collisional temperatures of T = 51 K and T = 125 K (with [He] = 1.6 × 1013 cm−3 and [He] = 2.1 × 1013 cm−3, respectively). The corresponding values of the binary reaction rate coefficients ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}-\mathrm{HD}}﹩ (indicated in the figure) are given by the slope of the plotted dependencies (see the text). The horizontal error bars indicate the estimated uncertainty in the pressure measurement. The statistical uncertainty of single rate measurement is smaller than the point size in this plot.
Paper: Reaction of N+ Ion with H2, HD, and D2 at Low Temperatures: Experimental Study of the Pathway to Deuterated Nitrogen-containing Molecules in the Interstellar Medium
Authors: Radek Plašil, Štěpán Roučka, Artem Kovalenko, Thuy Dung Tran, Serhiy Rednyk, Petr Dohnal, Dmytro Shapko, Dieter Gerlich, Juraj Glosík
Figure caption: Arrhenius plot of the temperature dependence of the rate coefficient ﹩{k}_{{{\rm{N}}}^{+}}^{{{\rm{D}}}_{2}}﹩ of the reaction of N+ with D2. The data obtained after correction of the measured ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{{\rm{D}}}_{2}}﹩ for the presence of HD in the D2 gas (closed circles) are fitted by the Arrhenius function with a background term (full line; see text). The raw uncorrected data of ﹩{k}_{{{\rm{N}}}^{+}}^{{\rm{g}}\text{-}{{\rm{D}}}_{2}}﹩ without binning are indicated with the small points. The data obtained in previous experiments by Marquette et al. (1988; CRESU), Gerlich (1993; 22PT), Ervin & Armentrout (1987; GIB), and Adams & Smith (1985; SIFDT) are shown for comparison.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: An example of a successful fit to a simulated SN Ia at z ≈ 2.2 that does not include any blended host galaxy light. (a) Corner plot for the sampled parameter space, where the red lines indicate truth values. The values and uncertainties on top of the panels indicate the estimates from the MCMC sampling. (b) Extracted spectrum in black, with gray errors, and 200 randomly drawn models, in magenta, from the posterior distribution within ±1σ of the inferred estimates. The input template for the SN is shown in blue. (c) Trace plot for the MCMC walkers, where red lines again indicate truth values. From top to bottom the subpanels are redshift, phase, and A  V . The exposure time is 1 hr for the extracted 1D spectrum.
Paper: High-precision Redshifts for Type Ia Supernovae with the Nancy Grace Roman Space Telescope P127 Prism
Authors: Bhavin A. Joshi, Louis-Gregory Strolger, Russell E. Ryan, Alexei V. Filippenko, Rebekah Hounsell, Patrick L. Kelly, Richard Kessler, Phillip Macias, Benjamin Rose, Daniel Scolnic
Figure caption: Same as Figure 9, but for an unsuccessful fit due to blended host galaxy light. The extracted 1D spectrum for the host galaxy is also shown (red line) as a reference for the spectrum that is blended with the SN input template. The true values are z true = 0.5288, phasetrue = 3 days, and ﹩{A}_{V}^{\mathrm{true}}=0.02﹩ mag. The inferred values are z = 0.038, phase = 3.91 days, and A  V  = 3.57 mag (also indicated on the corner plot).
Paper: The Star Formation Rate of the Milky Way as Seen by Herschel
Authors: D. Elia, S. Molinari, E. Schisano, J. D. Soler, M. Merello, D. Russeil, M. Veneziani, A. Zavagno, A. Noriega-Crespo, L. Olmi, M. Benedettini, P. Hennebelle, R. S. Klessen, S. Leurini, R. Paladini, S. Pezzuto, A. Traficante, D. J. Eden, P. G. Martin, M. Sormani, A. Coletta, T. Colman, R. Plume, Y. Maruccia, C. Mininni, S. J. Liu
Figure caption: Top: distributions of Hi-GAL protostellar clumps with and without a heliocentric distance estimate (black and red histograms, respectively) in 5° wide bins of Galactic longitude. Bottom: number ratio between protostellar clumps without a distance estimate and the total number, in the same longitude bins as in the top panel.
Paper: Deep Narrowband Photometry of the M101 Group: Strong-line Abundances of 720 H II Regions
Authors: Ray Garner, J. Christopher Mihos, Paul Harding, Aaron E. Watkins, Stacy S. McGaugh
Figure caption:  The narrowband filters used to image the M101 Group overlaid on a synthetic H II region spectrum from CIGALE. Top: the [O II] filters. Middle: the Hβ and [O III] filters. Bottom: the Hα filters. In all cases, the on-band filter sits on top of their respective emission lines, while the off-band filter sits redward of the emission line except for the Hβ-off filter which sits blueward. Particular emission and absorption lines are marked by vertical lines.
Paper: Deep Narrowband Photometry of the M101 Group: Strong-line Abundances of 720 H II Regions
Authors: Ray Garner, J. Christopher Mihos, Paul Harding, Aaron E. Watkins, Stacy S. McGaugh
Figure caption: The [N II]/[S II] residuals as a function of radius. Colored points indicate the survey: CHAOS (Croxall et al. 2016; green), Li et al. (2013; orange), and Kennicutt & Garnett (1996; blue). The solid black line indicates the best fit to the data within 1.25R 25, with the adjoining solid gray lines showing the 1σ uncertainty.
Paper: Deep Narrowband Photometry of the M101 Group: Strong-line Abundances of 720 H II Regions
Authors: Ray Garner, J. Christopher Mihos, Paul Harding, Aaron E. Watkins, Stacy S. McGaugh
Figure caption:  A color–magnitude diagram for sources in the 2MASS All-Sky Catalog of Point Sources (Skrutskie et al. 2006) within a 30′ × 30′ cutout centered on M101. Sources are colored according to their Hα EW. The box indicated by the solid black lines indicates those sources that are consistent with stars that we subsequently mask in our segmentation routine.
Paper: Deep Narrowband Photometry of the M101 Group: Strong-line Abundances of 720 H II Regions
Authors: Ray Garner, J. Christopher Mihos, Paul Harding, Aaron E. Watkins, Stacy S. McGaugh
Figure caption: Segmentation maps for M101 (left), NGC 5477 (top right), and NGC 5474 (bottom right). Each shaded region is a detected H II region after star removal and deblending as described in the text. The M101 map measures 30′ × 30′, the NGC 5477 map measures 5′ × 5′, and the NGC 5474 map measures 10′ × 10′. In all images, north is up and east is to the left.
Paper: Deep Narrowband Photometry of the M101 Group: Strong-line Abundances of 720 H II Regions
Authors: Ray Garner, J. Christopher Mihos, Paul Harding, Aaron E. Watkins, Stacy S. McGaugh
Figure caption: The M101–NGC 5474 interaction from the Linden model. Time progresses from left to right, top to bottom. The orbit of NGC 5474 is traced in black, and the stars in both galaxies are colored by local density of points. The red circle is of radius 2 kpc centered on the center of M101. Negative time indicates time before closest approach (∼14 kpc), and the bottom right panel shows the current-day arrangement of the galaxies.
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: Comparison between observed line fluxes and those predicted by the wind model (solid lines) as a function of the upper level number for the transition n upp. Solid symbols denote measurements from the IRTF/SpeX data, while open symbols are from Benedettini et al. (2001). Dotted lines are Case B values for T = 10,000 K, n  e  = 1.0 × 102 cm−3, reddened by A  V  = 8.1 mag, and scaled to match the observed Pa β flux, while the dashed lines are similarly Case B values for n  e  = 1.0 × 1010 cm−3.
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: (a) Center of the FORCAST three-color image on an asinh intensity scale; (b) simulated image for the best-fit parameters found in this work (PA = 197° and i = 55°) on the same intensity scale; (c) simulated image generated for PA ∼56° and i ∼ 15°, as found by Malbet et al. (2007); (d) simulated image generated for PA ∼120° and i ∼ 40°, as found by Acke et al. (2008).
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: Comparison between the continuum-subtracted IRTF/SpeX spectrum and the best-fitting wind model (red). Only H lines have been synthesized in the model.
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: Radial profile of the electron density (left-hand scale) and wind velocity (right-hand scale) in the H line emitting region for our best-fit parameters and the adopted wind model.
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: The 350 μm SPIRE image shows that MWC 297 is located on the southwestern rim of a small cloud. The emission at 350 μm is dominated by a prestellar core about 15″ northeast of the star. The gap to the southwest of the star is also seen in the 13CO(1–0) image by Ridge et al. (2003).
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: Integrated 13CO(1–0) emission plotted in color with 110 GHz continuum emission overlaid with red contours.
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: Re-reduced VLA CnD observations at 6.0 and 3.6 cm. The beam, which is very elliptical, is drawn in the lower right corner of each image.
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: VLA 6 cm image (contours) overlaid on a logarithmically stretched FORCAST 31.5 μm image in color. The VLA beam is plotted at the bottom right.
Paper: Multiwavelength Observations of MWC 297: Constraints on Disk Inclination and Mass Outflow
Authors: William D. Vacca, Göran Sandell
Figure caption: (Left) Dust temperature map derived from the FORCAST data. The contour around the bright yellow/orange region in the map corresponds to T ≈ 67 K. (right) Azimuthally averaged radial profile of the dust temperature.
Paper: Effects of Active Galactic Nucleus Feedback on Cold Gas Depletion and Quenching of Central Galaxies
Authors: Wenlin Ma, Kexin Liu, Hong Guo, Weiguang Cui, Michael G. Jones, Jing Wang, Le Zhang, Romeel Davé
Figure caption: Distribution of central galaxies as a function of SFR and M *. Each panel from left to right is Illustris, TNG, and SIMBA, respectively. The bins are color coded by the logarithmic number of galaxies. Black lines are the SFMS for Illustris and TNG, while black dots are shown in SIMBA. Red dotted lines are the separation of star-forming and quenched populations for all simulations (Equations (13)–(15)). The observed SFMS of G21 is shown as the blue dashed line in each panel.
Paper: A Panchromatic Study of Massive Stars in the Extremely Metal-poor Local Group Dwarf Galaxy Leo A 
Authors: Maude Gull, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi Choi, Anna F. McLeod, Kareem El-Badry, Ylva Götberg, Karoline M. Gilbert, Martha Boyer, Julianne J. Dalcanton, Puragra GuhaThakurta, Steven Goldman, Paola Marigo, Kristen B. W. McQuinn, Giada Pastorelli, Daniel P. Stark, Evan Skillman, Yuan-sen Ting, Benjamin F. Williams
Figure caption: Select HST-based UV-optical (left), near-UV (NUV)-optical (left middle), optical-only (right middle), and NIR (right) CMDs of Leo A. Colored points indicate stars observed with LRIS (Keck; navy triangles), Binospec (MMT; red dots), and both telescopes (magenta squares). For reference, we overplot select MIST tracks ([Fe/H] = −1.0, v/vcrit = 0.4, A  v  = 0.03). There are fewer stars on the NIR CMD because WFC3/IR has a smaller field of view and does not entirely overlap the UV and optical imaging. All spectroscopic stars are massive stars (i.e., M > 8M ⊙). The NUV CMD shows that the stars in our spectroscopic sample are not very evolved.
Paper: A Panchromatic Study of Massive Stars in the Extremely Metal-poor Local Group Dwarf Galaxy Leo A 
Authors: Maude Gull, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi Choi, Anna F. McLeod, Kareem El-Badry, Ylva Götberg, Karoline M. Gilbert, Martha Boyer, Julianne J. Dalcanton, Puragra GuhaThakurta, Steven Goldman, Paola Marigo, Kristen B. W. McQuinn, Giada Pastorelli, Daniel P. Stark, Evan Skillman, Yuan-sen Ting, Benjamin F. Williams
Figure caption: The Leo A HST ACS/F475W image zoomed in on the central region of the galaxy. Stars with spectroscopic observations are color-coded by telescope: Keck/LRIS (blue triangles), MMT/Binospec (red circles), and both (magenta squares). Contours of Hα emission from ground-based imaging (Local Volume Legacy Survey; Kennicutt et al. 2007) are overplotted in green. Note that many of the massive stars are not obviously associated with cataloged H II regions including one O-star (K7).
Paper: A Panchromatic Study of Massive Stars in the Extremely Metal-poor Local Group Dwarf Galaxy Leo A 
Authors: Maude Gull, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi Choi, Anna F. McLeod, Kareem El-Badry, Ylva Götberg, Karoline M. Gilbert, Martha Boyer, Julianne J. Dalcanton, Puragra GuhaThakurta, Steven Goldman, Paola Marigo, Kristen B. W. McQuinn, Giada Pastorelli, Daniel P. Stark, Evan Skillman, Yuan-sen Ting, Benjamin F. Williams
Figure caption: Example normalized spectra of massive stars in Leo A shown from 4000–5100 Å with key features labeled. Top two panels: Keck/LRIS (R ∼ 1800) spectra of an O-type (top) and a Be-type star (bottom) in Leo A. The O-star exhibits He I (dark blue) and He II (light blue) absorption lines and a clear Balmer series in absorption. These are typical of a late-type O star. The Be star shows He I (dark blue) absorption but no He II (light blue). The Balmer series is primarily in emission. Bottom two panels: Binospec spectra (R ∼ 1250) of an early B-type (top) and a B(e)-type (bottom) in Leo A. The B star shows primarily He I (dark blue) absorption features, while He II (light blue) absorption is minimal. The Balmer lines show absorption features, although there appears to be weak emission within the feature. The bottom panel shows a B0.5-type star. Though the low S/N makes identification of clear features more challenging, we still find clear He I (dark blue) absorption features. The Balmer lines are a mix of absorption and emission features. We note the star is potentially a Be star as well.
Paper: A Panchromatic Study of Massive Stars in the Extremely Metal-poor Local Group Dwarf Galaxy Leo A 
Authors: Maude Gull, Daniel R. Weisz, Peter Senchyna, Nathan R. Sandford, Yumi Choi, Anna F. McLeod, Kareem El-Badry, Ylva Götberg, Karoline M. Gilbert, Martha Boyer, Julianne J. Dalcanton, Puragra GuhaThakurta, Steven Goldman, Paola Marigo, Kristen B. W. McQuinn, Giada Pastorelli, Daniel P. Stark, Evan Skillman, Yuan-sen Ting, Benjamin F. Williams
Figure caption: This plot is identical to Figure 1, only zoomed in on luminous blue stars selected for spectroscopy in the UV and optical CMDs. We label the stars by the names in Table 1, where K stands for stars with Keck and B for stars with Binospec spectra. For reference, we overplot select MIST tracks ([Fe/H] = −1.0, v/vcrit = 0.4, A  v  = 0.03). Interestingly, a handful of stars that appear on the main sequence in the UV-optical CMDs appear in the blue core helium burning region of the F475W-F814W CMD. We discuss this in Section 5.3.
Paper: Effects of Active Galactic Nucleus Feedback on Cold Gas Depletion and Quenching of Central Galaxies
Authors: Wenlin Ma, Kexin Liu, Hong Guo, Weiguang Cui, Michael G. Jones, Jing Wang, Le Zhang, Romeel Davé
Figure caption: Similar to Figure 9, but for the dependences of ΔlogM HI,2R half , ﹩{\rm{\Delta }}\mathrm{log}\,{M}_{{{\rm{H}}}_{2},2{R}_{\mathrm{half}}}﹩, and ﹩{\rm{\Delta }}\mathrm{log}\,\mathrm{SFR}﹩ on ﹩{\rm{\Delta }}\mathrm{log}\,{{\rm{\Sigma }}}_{1}﹩ in TNG50. The measurements of TNG50 (circles) are compared with the observations of xGASS, xCOLD GASS, and G21. We also show the corresponding measurements of M HI and ﹩{M}_{{{\rm{H}}}_{2}}﹩ in TNG50 as the squares for comparison.
Paper: Effects of Active Galactic Nucleus Feedback on Cold Gas Depletion and Quenching of Central Galaxies
Authors: Wenlin Ma, Kexin Liu, Hong Guo, Weiguang Cui, Michael G. Jones, Jing Wang, Le Zhang, Romeel Davé
Figure caption: The trends of HIMS (left panel) and H2MS (right panel) for five H I /H2 transition models in TNG. Compared to Figure 3, we show the K13 model, which we used in this paper, as filled circles as fiducial data. The black solid line, green dotted line, purple dashed line, and red dashed–dotted line represent the GD14, GK11, L08, and S14 models, respectively.
Paper: Effects of Active Galactic Nucleus Feedback on Cold Gas Depletion and Quenching of Central Galaxies
Authors: Wenlin Ma, Kexin Liu, Hong Guo, Weiguang Cui, Michael G. Jones, Jing Wang, Le Zhang, Romeel Davé
Figure caption: Relation between ΔlogSFR and ΔlogMHI (left panel) and ﹩{\rm{\Delta }}{\mathrm{logM}}_{{{\rm{H}}}_{2}}﹩ (right panel) for five H I /H2 transition models in TNG. Labels are the same as in Figure 12. Similar to Figure 4, we show G21 and xCOLD GASS observational data for comparison.
Paper: Effects of Active Galactic Nucleus Feedback on Cold Gas Depletion and Quenching of Central Galaxies
Authors: Wenlin Ma, Kexin Liu, Hong Guo, Weiguang Cui, Michael G. Jones, Jing Wang, Le Zhang, Romeel Davé
Figure caption: Similar to Figure 9, we show the dependence of ΔlogMHI,2Rhalf  (top panels) and ﹩{\rm{\Delta }}{\mathrm{logM}}_{{{\rm{H}}}_{2},2{R}_{\mathrm{half}}}﹩ (bottom panels) on M BH (left panels) and f edd (right panels) for five H I /H2 transition models in TNG. Labels are the same as in Figure 12.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Histogram of the SAM M * vs. predicted M * with logarithmically colored bin heights. The left panel shows the target-prediction relation for our GNN, Mangrove, and the right panel shows the target–prediction relation of the common abundance matching approach. Kernel density estimates of the SAM and Mangrove-predicted distributions are shown on the relevant axes. By leveraging the formation history of the galaxy via the merger tree, we obtain precise and accurate predictions of M *. The prediction scatter is improved by almost a factor of two compared to the state-of-the-art, single-halo method and by more than a factor of 4 compared to the widely used abundance matching method (see Table 1). Mangrove's M * scatter is comparable to, but still well above, the probabilistic limit of the SAM, which is at 0.043 dex.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: An illustration of the full workflow of Mangrove. Merger trees are encoded as graphs, which are then passed through Mangrove. Messages are passed forward in time only, since merger trees are directed in time. Node states are updated by applying a learnable function f to the current node states, applying a learnable function g to the mean of the node states of the neighboring nodes, and adding these two as described in Section 3. Transferring into the latent space is marked by shaded colors and a change in shape from circles to rectangles. Adding neighborhood information is marked by a mixture of colors. The model makes message-passing steps, after which the graph nodes are summed over, and this sum is then decoded by another learnable function, h, which gives the predictions and the Gaussian covariance matrix. All learnable functions are MLPs.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Histogram of SAM targets vs. the predicted targets of our GNN, Mangrove, with logarithmically colored bin heights. Recovering galactic M cold, Z gas, SFR, SFR100, and M BH renders mostly tight and unbiased relationships across the entire ranges of these galactic features, with the notable exception of targets where SFR or SFR100 > 0.1. This flaw is spurious and should be possible to mitigate. All of these results outperform results from the literature for all precision metrics (see Table 1). The fact that such mappings exist implies that the full hyperplane of galactic properties may be emulated with Mangrove.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: The merger tree of a 108.5 M ⊙ galaxy. Only nodes that are progenitors, merging, or final (at z = 0) are shown. Both color and dot size encode the mass of the halos. The merger tree encodes the full formation history and temporally evolving dark matter features of all halos that merge to form the final halo. Galaxies co-evolve with their dark matter halo, and the dark matter merger trees are therefore useful for determining galaxy formation.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: A partial merger tree showing the merger tree from Figure 1 with the nodes with the 75% highest redshift pruned, which is our method of quantifying the importance of nodes at high redshifts. If our M * prediction from using this reduced tree is as good as when using the full tree, it indicates that there was no useful information in the 75% highest redshift nodes. The relation between precision and cutoff percentage can be seen in Figure 8.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Median and 16th/84th percentile of the scatter for 25 models at each percentile cut. There is a clear trend toward a loss of accuracy as we remove more nodes, so the stellar mass prediction depends strongly on the assembly history of the given galaxy. The curve is approximately exponential. Note, however, that the drop in accuracy when pruning the 50% highest redshift nodes is small.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Median and 16th/84th percentiles of 10 models trained to only predict M * at a series of different redshifts in three different ways. Red is when testing at the same single redshift where Mangrove was trained, black is from training and testing jointly at z ∈ 0, 0.5, 1, 2, and green is from training jointly at z ∈ 0, 0.5, 1, 2 and testing at z ∈ 0.25, 0.75, 1.5, and 1.75. Mangrove predicts M * at previously unseen redshifts with a similar or lower scatter than the redshifts at which Mangrove was trained.
Paper:  Mangrove: Learning Galaxy Properties from Merger Trees
Authors: Christian Kragh Jespersen, Miles Cranmer, Peter Melchior, Shirley Ho, Rachel S. Somerville, Austen Gabrielpillai
Figure caption: Same as Figure 4, but including a point from extrapolating to z = 3 using the models trained at z ∈ 0, 0.5, 1, 2. The predictions have much higher scatters.